Theoretical aspects of Dark Matter search · Carlos Muñoz UAM & IFT Dark Matter 3 Last results from the Planck satellite, W b h2 0.022 W DM h2 0.12 confirm that about 85% of the

Carlos Muñoz

Theoretical aspects of Dark Matter search

RICAP-13, Roma, May 22-24

Evidence for DM

Evidence for dark matter since 1930’s:

COBE, WMAP, Planck

Carlos Muñoz

UAM & IFT

Dark Matter 2

http://es.wikipedia.org/wiki/Archivo:WMAP.jpg

Carlos Muñoz

UAM & IFT

Dark Matter

3

Last results from the Planck satellite,

W b h2 0.022

W DM

h2 0.12

confirm that about 85% of the matter in the Universe is dark

W DE

h2 0.31

http://www.google.es/url?sa=i&rct=j&q=planck+results&source=images&cd=&cad=rja&docid=ssIUhldXVl-mTM&tbnid=J8QNwd9SqFBcBM:&ved=0CAUQjRw&url=http://blogs.discovermagazine.com/outthere/2013/03/22/four-surprises-in-plancks-new-map-of-the-cosmos/&ei=UdyPUeGZA4aG0AXisoHIBA&bvm=bv.46340616,d.ZGU&psig=AFQjCNFhrK95RyXfFg1f4FeagZfCjeXoLQ&ust=1368468918871780

Dark Matter

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The only possible candidate for DM within the Standard Model of Particle Physics, the neutrino, is excluded

Its mass seems to be too small, m ~ eV to account for W DM h2 0.1

This kind of (hot) DM cannot reproduce correctly the observed structure in the Universe; galaxies would be too young

This is a clear indication that we need to go

beyond the standard model of particle physics

PARTICLE CANDIDATES

Carlos Muñoz

UAM & IFT

We need a new particle with the following properties:

Stable or long-lived

Neutral Otherwise it would bind to nuclei and would be excluded from unsuccessful searches for exotic heavy isotopes

Produced after the Big Bang and still present today

Reproduce the observed amount of dark matter W DM h2 0.1

A stable and neutral WIMP is a good candidate for DM, since it is able to reproduce this number

5 Dark Matter

In the early Universe, at some temperature the annihilation rate of DM WIMPs dropped below the expansion rate

and their density has been the same since then, with:

Carlos Muñoz

UAM & IFT

h2 WIMP

sann = sweak

3 x 10-27 cm3 s-1

sannv 0.1

WIMP

WIMP

f

f

W

DIRECT DETECTION

r0 ~ 0.3 GeV/cm3

v0 ~ 220 km/s J ~ r0 v0 /mWIMP ~ 10

4 WIMPs /cm2 s

through elastic scattering with nuclei in a detector is possible

DAMA/LIBRA photo

For sWIMP-nucleon 10-8-10-6 pb a material with nuclei composed of about 100 nucleons, i.e. mN ~ 100 GeV

R ~ J sWIMP-nucleon/ mN 10-2 -1 events/kg day

EWIMP 1/2 (100 GeV/c2) (220 km/s)2 25 keV

energy produced by the recoiling nucleus can be measured through ionization, scintillation, heat few keV

Dark Matter

6 Carlos Muñoz

UAM & IFT

DIRECT DARK MATTER DETECTION

Superheated liquids (bubble)

Scintillation (light)

Ionization (charge)

Phonon (heat)

1. introduction Defensa de Tesis Doctoral Clara Cuesta Soria

PICASSO (C4F10) SIMPLE (C2ClF5) COUPP (CF3I)

DAMA/LIBRA (NaI) KIMS (CsI) XMASS (Xe) ANAIS (NaI) DM-Ice (NaI) DEAP3600 (Ar) MiniCLEAN (Ar)

XENON100 (Xe) ZEPLIN-III (Xe) LUX (Xe) XENON1T (Xe) ArDM (Ar) DarkSide (Ar)

CRESST (CaWO4) EURECA (CaWO4)

CUORE (TeO2)

CDMS (Ge, Si ) EDELWEISS-II (Ge) SuperCDMS (Ge) EURECA (Ge)

CoGeNT (Ge) TEXONO-CDEX (Ge) C-4 (Ge) DRIFT (CS2) DM-TPC (CF4) NEWAGE (CF4) MIMAC (3He/CF4) MAJORANA (Ge) GERDA (Ge)

Present Future DM hints

CRESST (CaWO4)

DAMA/LIBRA (NaI)

XENON10 (Xe)

CDMS (Si)

CoGeNT (Ge)

Dark Matter

8 Carlos Muñoz UAM & IFT

CRESST (CaWO4)

DAMA/LIBRA (NaI)

XENON10 (Xe)

CDMS (Si)

CoGeNT (Ge)

CMSSM (Buchmüller et al. 2012)

CMSSM + g-2 (Strege et al. 2012)

Neutralino in the (Constrained) MSSM

Supersymmetry

Dark Matter


CRESST (CaWO4)

DAMA/LIBRA (NaI)

XENON10 (Xe)

CDMS (Si)

CoGeNT (Ge)

Non-Universal Higgs (NUHM)

(Buchmüller et al. 2012)

NUHM+ g-2 (Strege et al. 2012)

Very light (Non-Universal Gauginos)

(Fornengo et al. 2013)

Neutralino in the MSSM – Unconstrained scenarios

Very light (Non-Universal

Gauginos) (Albornoz Vasquez

et al. 2011)

without the recent constrains on the Higgs sector, like the 125 GeV Mass, and the invisible Higgs decay

Dark Matter


Neutralino in the Next-to-MSSM (NMSSM)

Dark Matter


Light Bino-singlino neutralinos are possible The detection cross section can be larger (through the exchange of light Higgses)

W=µ H1 H2 N H1 H2

Right-handed sneutrinos can also be the dark matter in extensions of the NMSSM

N H1 H2 + N N c c

Whereas in the MSSM a LSP purely RH sneutrino implies scattering cross section too small, relic density too large, here the N provides efficient interactions of sneutrino too

~ c

~ c

(Cerdeño, Seto '09)

o Light sneutrinos are viable and distinct from MSSM neutralinos

o Viable, accessible and not yet excluded

(Cerdeño, C.M., Seto ‘08)

CRESST (CaWO4)

DAMA/LIBRA (NaI)

XENON10 (Xe)

CDMS (Si)

CoGeNT (Ge)

Right-handed sneutrino in the Next-to-MSSM

Very light RH Sneutrinos Cerdeno et al. 2011

Cerdeno et al. in preparation

Dark Matter


Annihilation of DM particles in the galactic halo will produce gamma rays, antimatter, neutrinos

and these can be measured in space–based detectors: Fermi (gammas), PAMELA, AMS (antimatter) or in Cherenkov telescopes:

MAGIC, HESS, VERITAS, CANGAROO (gammas) See talk by Doro

INDIRECT DETECTION

Also neutrino telescopes like ANTARES or ICECUBE can be used for detecting DM annihilation from the Sun, Earth or galactic center See talks by Zornoza & Taboada

Dark Matter

13 Carlos Muñoz

UAM & IFT

Dark Matter

14 Carlos Muñoz

UAM & IFT

Synchrotron emission from electrons and positrons generated by DM annihilation in the galactic halo, when interacting with the galactic magnetic field, can be measured in radio surveys

See talk by Lineros

e.g. an excess of antiparticles could be a signature of DM annihilations

problems with the DM explanation:

Otherwise we would have to require boost factors ranging between 102 and 104 provided by clumpiness in the dark matter distribution

Data implies σannv ~10–23 cm3 s–1 , but this would

produce

10 are not expected

Contributions of e– and e + from Geminga pulsar assuming different distance, age and energetic of the pulsar.

Possible astrophysical explanation:

No antiproton excess is observed , 2013 , 2008 , 2011

See talk by Battiston

But conventional astrophysics in the galactic center is not well understood. An excess might be due to the modeling of the diffuse emission, unresolved sources, etc.

an excess of gamma rays could be a signature of DM annihilations

An interesting possibility could be to search for DM around the Galactic Center where the density is very large Fermi-LAT: Morselli, Cañadas, Vitale, 2010 analized the inner galaxy region

Dark Matter

16 Carlos Muñoz

UAM & IFT

particle physics astrophysics

Assuming an excess, and that the DM density in the inner galaxy is r(r) ~ r0/r ,

one can deduce possible DM examples reproducing the observations

Hooper, Goodenough, 1010.2751 Hooper, Linden, 1110.0006

1.3

Dark Matter

17 Carlos Muñoz

UAM & IFT

7 x 10-27 cm3 s-1 sannv

But there are other possible explanations:

-Consistency of the excess with a millisecond pulsar population, Abazajian 1011.4275

-Cosmic-ray effects, Chernyakova 1009.2630

-Different spectrum of the point source at the galactic center, Boyarsky, Malyshev, Ruchayskiy, 1012.5839

Carlos Muñoz

UAM & IFT

18

Weniger, 1204.2797 presented a search for lines in the Fermi-LAT 43 month of data concentrating on energies between 20 - 300 GeV.

In regions close to the Galactic Center he found an indication for a gamma-ray line at an energy 130 GeV

If interpreted in terms of DM particles annihilating to a photon pair, the observations would imply mDM 130 GeV, σannv ~10

–27 cm3 s–1 when using Einasto profile

Dark Matter

Gamma-ray lines are traditional smoking gun signatures for DM annihilation

Local Group dwarf spheroidal galaxies (dSph) are attractive targets because:

-they are nearby -largely dark matter dominated systems -relatively free from gamma-ray emission from other astrophysical sources

But 24-month measurements of 10 dSph reported by Fermi-LAT show no excess 1108.3546

one can constrain DM particle properties:

WIMPs are ruled out to a mass of about

27 GeV for the bb channel

37 GeV for the +- channel 3 x 10-26 cm3 s-1 sannv

thermal cross section

19 Carlos Muñoz

UAM & IFT

Nearby clusters of galaxies are also attractive targets

-they are more distant, but more massive than dSphs -very dark matter dominated like dSphs -typically lie at high galactic latitudes where the contamination from galactic gamma-ray background emission is low

3-year Fermi-LAT data show no excess Han et al., 1207.6749:

Dark Matter

20 Carlos Muñoz

UAM & IFT

Adopting a boost factor of 103 from subhalos, WIMPs are ruled out to a mass of about 100 GeV for the bb and +- channels, and 10 GeV for the µ+µ- channel

Fermi-LAT, 1002.2239

Geringer-Sameth, Koushiappas, 1108.2914

Dark Matter

21 Carlos Muñoz

UAM & IFT

Fermi-LAT measurements of anisotropies in the diffuse gamma-ray background can also have implications for dark matter constraints See talk by Gómez-Vargas

Carlos Muñoz

UAM & IFT

Dark Matter 22

Is it possible to derive (even more) stringent constraints on parameters of generic DM candidates?

Let us analyze again the region around the Galactic Center,

YES in the likely case that the collapse of baryons to the Galactic Center is accompanied by the contraction of the DM

Cerdeño, Huh, Klypin, Mambrini, C.M., Peiró, Prada, MultiDark + Gómez-Vargas, Morselli, Sánchez-Conde Fermi-LAT

Preliminary results

The behaviour of NFW might be modified ρ 1/r making steeper: 1/r

Prada, Klypin, Flix Molina, Martinez, Simonneau, 0401512 Mambrini, Munoz, Nezri, Prada, 0506204

From observational data of the Milky Way, the parameters of the DM profiles have been

constrained. Fitting the data

in the inner region ρ 1/r in the inner region ρ 1/r1.37

Carlos Muñoz

UAM & IFT

23 Dark Matter

To set constraints we request that the expected DM signal does not exceed the observed flux (due to DM + astrophysical background)

No subtraction of any astrophysical background is made. Very conservative analysis!

to be compared with the observations

4-year Fermi-LAT data

mDM > 681 GeV mDM > 157-439 GeV

mDM > 531 GeV mDM > 489 GeV

In general the final state will be a combination of the final states presented here

e.g., in SUSY, the neutralino annihilation modes are 70% bb - 30% for a Bino DM, and 100% W+W- for a Wino DM

Also, the value of sv in the Galactic halo might be smaller than 3 x10-26 cm3 s-1

-e.g., in SUSY, in the early Universe coannihilation channels can also contribute to sv -Also, DM particles whose annihilation in the Early Universe is dominated by velocity dependent contributions would have a smaller value of sv in the Galactic halo,

where the DM velocity is much smaller, and can escape this constraint:

In this sense, the results derived for pure annihilation channels can be interpreted as limiting cases which give an idea of what can happen in realistic scenarios

But still Fermi-LAT data imply that large regions of parameters of DM candidates are not compatible with compressed DM density profiles

Work in progress, Constraining the SUSY parameter space inspired by an old study of the MSSM:

Carlos Muñoz

UAM & IFT

25 Dark Matter

Mambrini, Munoz, Nezri, Prada, 0506204

So we are now updating the neutralino MSSM case and studying the NMSSM, and the sneutrino in the extension of the NMSSM

Cerdeño, Gómez-Vargas, Huh, Klypin, Mambrini, Morselli, C.M., Peiró, Prada, Sánchez-Conde

in preparation

Gravitino as decaying dark matter

neutralino, sneutrino, …, but also the gravitino might be a good candidate and detectable

In models where R-parity is broken, the neutralino or the sneutrino with very short lifetimes cannot be used as candidates for dark matter

Nevertheless, the gravitino (superWIMP) can be a good candidate

Its decay is supressed both by the Planck mass and the small R-parity breaking,

thus the lifetime of the gravitino can be longer than the age of the Universe (1017 s)

Takayama, Yamaguchi, 2000

Carlos Muñoz

UAM & IFT

26 Dark Matter

FERMI might in principle detect these gamma rays

Buchmuller, Covi, Hamaguchi, Ibarra, Yanagida, 07

Bertone, Buchmuller, Covi, Ibarra, 07

Ibarra, Tran, 08

Ishiwata, Matsumoto, Moroi, 08

Since the gravitino decays into a photon and neutrino, the former produces a monochromatic line at energies equal to m3/2/2

SSM

López-Fogliani, C.M, 05

Constraints on SSM gravitino DM analyzed in

Choi, López-Fogliani, C.M., Ruiz de Austri, 0906.3681

Gómez-Vargas, Fornasa, Zandanel, Cuesta, C.M., Prada, Yepes, 1110.3305

Carlos Muñoz

UAM & IFT

27 Dark Matter

10º x 10º region around the GC

DM

In the SSM: U g1 /M1 10-6 – 10-8

Values of the gravitino mass larger than 4 GeV are disfavoured, as well as lifetimes smaller than about 3 x 1027 s.

Unconstrained regions

Conclusions

Thus the present experimental situation is very exciting.

There are impressive experimental efforts by many groups around the world to detect the dark matter:

So, stay tuned !

And, besides, the LHC is working

DAMA/LIBRA, CoGeNT, CRESST, CDMS, XENON,…, Fermi, PAMELA, AMS, etc.

Carlos Muñoz

UAM & IFT

29 Dark Matter

BACK UP SLICES

DM constraints from Fermi-LAT 32 Carlos Muñoz

UAM & IFT

But these are DM-only simulations, and central regions of galaxies like the Milky Way are dominated by baryons

They might modify e.g. the behaviour of NFW ρ 1/r making it steeper

The baryons lose energy through radiative processes and fall into the central regions of a forming galaxy. Thus the resulting gravitational potential is deeper, and the DM must move closer to the center increasing its density

Zeldovich, Klypin, Khlopov, Chechetkin, 1980 Blumenthal, Faber, Flores, Primack, 1986 Gnedin, Kravtsov, Klypin, Nagai, 0406247

The effect seems to be confirmed by high-resolution hydrodynamic simulations that self-consistently include complex baryonic physics such as gas dissipation, star formation and supernova feedback

Gustafsson, Fairbairn, Sommmer-Larsen, 0608634 Colín, Valenzuela, Klypin, 0506627 Tissera, White, Pedrosa, Scannapieco, 0911.2316 O.Y. Gnedin, Ceverino, N.Y. Gnedin, Klypin, Kravtsov, Levine, Nagai, Yepes, 1108.5736

Carlos Muñoz

UAM & IFT

33 DM constraints from Fermi-LAT

Caution:

Astrophysicists identified another process, which tends to decrease the DM density and flatten the DM cusp

Mashchenko, Couchman, Wadsley, 0605672, 0711.4803 Pontzen, Governato, Blumenthal, 1106.0499

The mechanism relies on numerous episodes of baryon infall followed by a strong burst of star formation, which expels the baryons producing at the end a significant decline of the DM density.

Cosmological simulations which implement this process show this result

Governato et al., 0911.2237 Maccio et al, 1111.5620

Whether the process happened in reality in the Milky Way is still unclear…

Documents

Theoretical aspects of Dark Matter search · Carlos Muñoz UAM & IFT Dark Matter 3 Last results from the Planck satellite, W b h2 0.022 W DM h2 0.12 confirm that about 85% of the